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Selected 7% of my papers with unique contributions:
- The suggestion that jets launched during the AGB to PN transition (Asymptotic Giant Branch to Planetary Nebula transition) form the two opposite optical bright knots observed in elliptical planetary nebulae was mentioned in Soker (1990) .
- The idea that planets shape planetary nebulae in a non-negligible number of cases was raised by me in 1991, and was discussed in depth in Soker (1996) and some later papers.
- The idea that planets lead to the formation of some sdB stars (blue horizontal branch stars) was suggested in Soker (1998).
- The accretion model for the 19th century Great Eruption of Eta Carinae was suggested in Soker (2001) and studied in Kashi & Soker (2010).
- The mergerburst model, where two main-sequence stars merge, for the outburst of V838 Monocerotis was put forward by Soker & Tylenda (2003) .
- The cold feedback mechanism in cooling flows in clusters of galaxies and in galaxies was suggested by Pizzolato & Soker (2005).
- The jittering-jet mechanism for exploding all core collapse supernovae (massive stars) was suggested by Papish & Soker (2011).
- The core-degenerate scenario for forming the progenitors of Type Ia supernovae (SN Ia) was suggested by Kashi & Soker (2011) .
- A review on the jet feedback mechanism (JFM) in different astrophysical objects is given by Soker, Akashi, Gilkis, Hillel, Papish, Refaelovich, & Tsebrenko (2013), and in Soker (2016).
- The mixing-heating process, where bubbles in cooling flows heat the intra-cluster medium by mixing was demonstrated by Gilkis & Soker (2013) and Hillel & Soker (2014).
- The proposition that in many cases jets facilitate common envelope (CE) ejection, in particular when the CE is terminated by migration, was put forward in Soker (2014).
- The Grazing Envelope Evolution (GEE) is an evolutionary channel that can replace the CE evolution in forming close binary systems (Soker 2015). In the GEE the binary system might be viewed as evolving in a constant state of `just entering a CE phase’.
- The claim that many SN Ia are SNIPs (SNe Inside Planetary nebulae) was made by Tsebrernko & Soker (2015).
- A new process where a binary system breaks up inside a common envelope was introduced by Sabach & Soker (2015) to explain the formation of the triple pulsar PSR J0337+1715.
- The transient objects in the gap between novae and supernovae, collectively termed intermediate luminosity optical transients (ILOTs), were classified into three groups by Kashi & Soker (2015). We further developed the high-accretion-powered ILOT model (the HAPI model) to account for the high ILOT luminosity, and argued that in many cases the jets operate through the negative jet-feedback mechanism (JFM).
- I suggested (Soker 2016) that the main process that amplifies magnetic fields in cooling flows in clusters and group of galaxies is a jet-driven dynamo (JEDD). The main processes that are behind the JEDD are the turbulence and the large scale shear formed by the propagating jet.
- We (Soker & Gilkies 2017) proposed that a dynamo amplification of magnetic fields in the core of massive stars takes place tens of years to hours before they explode. Such a dynamo might cause envelope expansion and enhanced mass-loss rate, resulting in pre-explosion outbursts (PEOs) when an interaction with a binary companion takes place.
- We (Soker & Gilkis 2018) proposed that the enigmatic supernova iPTF14hls can be explained by a common envelope jets supernova (CEJSN) scenario. In the CEJSN a neutron star that spirals-in inside the envelope of a massive giant star accretes mass and launches jets that power the ejection of the circumstellar shell and later the explosion itself.
- We (Grichener & Soker 2019) solidified an early suggestion (Papish, Soker, & Bukay 2015) that the heavy r-process elements are synthesized in the jets of common envelope jets supernovae. This is termed the CEJSN r-process scenario.
- We (Sabach & Soker 2018) suggested that stars whose angular momentum (J) does not increase by a companion, star or planet, along their post-main sequence evolution have much lower mass loss rates along their giant branches, an dhence they deserve a class of their own, which we term Jsolated stars.
- I (Soker 2019) proposed the possiblity that in rare cases Type Ia supernovae evaporate a planet.
- Ealeal Bear and I (Bear & Soker 2020) proposed that in very rare cases a triple stellar system can lead to a core collapse supernova inside a planetary nebula (CCSNIP). For that, the whit edwarf forms before the neutron star is born, in what is termed a white dwarf – neutron star reverse evolution (Sabach & Soker 2014).